Most of the post-Jupiter voyage was spent in hibernation mode to preserve on-board systems, except for brief annual checkouts.[13] On December 6, 2014, New Horizons was brought back online for the Pluto encounter, and instrument check-out began.[14] On January 15, 2015, the New Horizons spacecraft began its approach phase to Pluto.

In August 1992, JPL scientist Robert Staehle called Pluto discoverer Clyde Tombaugh, requesting permission to visit his planet. "I told him he was welcome to it," Tombaugh later remembered, "though he's got to go one long, cold trip."[25] The call eventually led to a series of proposed Pluto missions, leading up to New Horizons.

Stamatios "Tom" Krimigis, head of the Applied Physics Laboratory's space division, one of many entrants in the New Frontiers Program competition, formed the New Horizons team with Alan Stern in December 2000. Appointed as the project's principal investigator, Stern was described by Krimigis as "the personification of the Pluto mission".[26]New Horizons was based largely on Stern's work since Pluto 350 and involved most of the team from Pluto Kuiper Express.[27] The New Horizons proposal was one of five that were officially submitted to NASA. It was later selected as one of two finalists to be subject to a three-month concept study, in June 2001. The other finalist, POSSE (Pluto and Outer Solar System Explorer), was a separate, but similar Pluto mission concept by the University of Colorado Boulder, led by principal investigator Larry W. Esposito, and supported by the JPL, Lockheed Martin and the University of California.[28] However, the APL, in addition to being supported by Pluto Kuiper Express developers at the Goddard Space Flight Center and Stanford University,[28] were at an advantage; they had recently developed NEAR Shoemaker for NASA, which had successfully entered orbit around 433 Eros earlier in the year, and would later land on the asteroid to scientific and engineering fanfare.[29]

In November 2001, New Horizons was officially selected for funding as part of the New Frontiers program.[30] However, the new NASA Administrator appointed by the Bush Administration, Sean O'Keefe, was not supportive of New Horizons, and effectively cancelled it by not including it in NASA's budget for 2003. NASA's Associate Administrator for the Science Mission Directorate Ed Weiler prompted Stern to lobby for the funding of New Horizons in hopes of the mission appearing in the Planetary Science Decadal Survey; a prioritized "wish list", compiled by the United States National Research Council, that reflects the opinions of the scientific community. After an intense campaign to gain support for New Horizons, the Planetary Science Decadal Survey of 2003–2013 was published in the summer of 2002. New Horizons topped the list of projects considered the highest priority among the scientific community in the medium-size category; ahead of missions to the Moon, and even Jupiter. Weiler stated that it was a result that "[his] administration was not going to fight".[26] Funding for the mission was finally secured following the publication of the report, and Stern's team were finally able to start building the spacecraft and its instruments, with a planned launch in January 2006 and arrival at Pluto in 2015.[26]Alice Bowman became Mission Operations Manager.[31]

New Horizons is the first mission in NASA's New Frontiers mission category, larger and more expensive than the Discovery missions but smaller than the Flagship Program. The cost of the mission (including spacecraft and instrument development, launch vehicle, mission operations, data analysis, and education/public outreach) is approximately $700 million over 15 years (2001–2016).[32] The spacecraft was built primarily by Southwest Research Institute (SwRI) and the Johns Hopkins Applied Physics Laboratory. The mission's principal investigator is Alan Stern of the Southwest Research Institute (formerly NASA Associate Administrator).

After separation from the launch vehicle, overall control was taken by Mission Operations Center (MOC) at the Applied Physics Laboratory in Howard County, Maryland. The science instruments are operated at Clyde Tombaugh Science Operations Center (T-SOC) in Boulder, Colorado.[33] Navigation is performed at various contractor facilities, whereas the navigational positional data and related celestial reference frames are provided by the Naval Observatory Flagstaff Station through Headquarters NASA and JPL; KinetX is the lead on the New Horizons navigation team and is responsible for planning trajectory adjustments as the spacecraft speeds toward the outer Solar System. Coincidentally the Naval Observatory Flagstaff Station was where the photographic plates were taken for the discovery of Pluto's moon Charon; and the Naval Observatory is itself not far from the Lowell Observatory where Pluto was discovered.

New Horizons was originally planned as a voyage to the only unexplored planet in the SolarSystem. When the spacecraft was launched, Pluto was still classified as a planet, later to be reclassified as a dwarf planet by the International Astronomical Union (IAU). Some members of the New Horizons team, including Alan Stern, disagree with the IAU definition and still describe Pluto as the ninth planet.[34] Pluto's satellites Nix and Hydra also have a connection with the spacecraft: the first letters of their names (N and H) are the initials of New Horizons. The moons' discoverers chose these names for this reason, plus Nix and Hydra's relationship to the mythological Pluto.[35]

About 30 grams (1 oz) of Clyde Tombaugh's ashes are aboard the spacecraft, to commemorate his discovery of Pluto in 1930.[41][42] A Florida-state quarter coin, whose design commemorates human exploration, is included, officially as a trim weight.[43] One of the science packages (a dust counter) is named after Venetia Burney, who, as a child, suggested the name "Pluto" after its discovery.

The goal of the mission is to understand the formation of the Plutonian system, the Kuiper belt, and the transformation of the early Solar System.[44] The spacecraft collected data on the atmospheres, surfaces, interiors, and environments of Pluto and its moons. It will also study other objects in the Kuiper belt.[45] "By way of comparison, New Horizons gathered 5,000 times as much data at Pluto as Mariner did at the Red Planet."[46]

Some of the questions the mission attempts to answer are: What is Pluto's atmosphere made of and how does it behave? What does its surface look like? Are there large geological structures? How do solar wind particles interact with Pluto's atmosphere?[47]

The spacecraft is comparable in size and general shape to a grand piano and has been compared to a piano glued to a cocktail bar-sized satellite dish.[49] As a point of departure, the team took inspiration from the Ulysses spacecraft,[50] which also carried a radioisotope thermoelectric generator (RTG) and dish on a box-in-box structure through the outer Solar System. Many subsystems and components have flight heritage from APL's CONTOUR spacecraft, which in turn had heritage from APL's TIMED spacecraft.

New Horizons' body forms a triangle, almost 0.76 m (2.5 ft) thick. (The Pioneers have hexagonal bodies, whereas the Voyagers, Galileo, and Cassini–Huygens have decagonal, hollow bodies.) A 7075 aluminium alloy tube forms the main structural column, between the launch vehicle adapter ring at the "rear," and the 2.1 m (6 ft 11 in) radio dish antenna affixed to the "front" flat side. The titanium fuel tank is in this tube. The RTG attaches with a 4-sided titanium mount resembling a gray pyramid or stepstool. Titanium provides strength and thermal isolation. The rest of the triangle is primarily sandwich panels of thin aluminium facesheet (less than 1⁄64 in or 0.40 mm) bonded to aluminium honeycomb core. The structure is larger than strictly necessary, with empty space inside. The structure is designed to act as shielding, reducing electronics errors caused by radiation from the RTG. Also, the mass distribution required for a spinning spacecraft demands a wider triangle.

The interior structure is painted black to equalize temperature by radiative heat transfer. Overall, the spacecraft is thoroughly blanketed to retain heat. Unlike the Pioneers and Voyagers, the radio dish is also enclosed in blankets that extend to the body. The heat from the RTG adds warmth to the spacecraft while it is in the outer Solar System. While in the inner Solar System, the spacecraft must prevent overheating, hence electronic activity is limited, power is diverted to shunts with attached radiators, and louvers are opened to radiate excess heat. While the spacecraft is cruising inactively in the cold outer Solar System, the louvers are closed, and the shunt regulator reroutes power to electric heaters.

New Horizons has both spin-stabilized (cruise) and three-axis stabilized (science) modes controlled entirely with hydrazinemonopropellant. Additional post launch delta-v of over 290 m/s (1,000 km/h; 650 mph) is provided by a 77 kg (170 lb) internal tank. Helium is used as a pressurant, with an elastomeric diaphragm assisting expulsion. The spacecraft's on-orbit mass including fuel is over 470 kg (1,040 lb) on the Jupiter flyby trajectory, but would have been only 445 kg (981 lb) for the backup direct flight option to Pluto. Significantly, had the backup option been taken, this would have meant less fuel for later Kuiper belt operations.

There are 16 thrusters on New Horizons: four 4.4 N (1.0 lbf) and twelve 0.9 N (0.2 lbf) plumbed into redundant branches. The larger thrusters are used primarily for trajectory corrections, and the small ones (previously used on Cassini and the Voyager spacecraft) are used primarily for attitude control and spinup/spindown maneuvers. Two star cameras are used to measure the spacecraft attitude. They are mounted on the face of the spacecraft and provide attitude information while in spin-stabilized or 3-axis mode. In between the time of star camera readings, spacecraft orientation is provided by dual redundant miniature inertial measurement units. Each unit contains three solid-state gyroscopes and three accelerometers. Two Adcole Sun sensors provide attitude determination. One detects the angle to the Sun, whereas the other measures spin rate and clocking.

A cylindrical radioisotope thermoelectric generator (RTG) protrudes in the plane of the triangle from one vertex of the triangle. The RTG provided 7002245700000000000♠245.7 W of power at launch, and was predicted to drop approximately 5% every 4years, decaying to 7002200000000000000♠200 W by the time of its encounter with the Plutonian system in 2015 and will decay too far to power the transmitters in the 2030s.[4] There are no onboard batteries. RTG output is relatively predictable; load transients are handled by a capacitor bank and fast circuit breakers.

The RTG, model "GPHS-RTG," was originally a spare from the Cassini mission. The RTG contains 9.75 kg (21.5 lb) of plutonium-238 oxide pellets.[27] Each pellet is clad in iridium, then encased in a graphite shell. It was developed by the U.S. Department of Energy at the Materials and Fuels Complex, a part of the Idaho National Laboratory.[51]
The original RTG design called for 10.9 kg (24 lb) of plutonium, but a unit less powerful than the original design goal was produced because of delays at the United States Department of Energy, including security activities, that delayed plutonium production.[52] The mission parameters and observation sequence had to be modified for the reduced wattage; still, not all instruments can operate simultaneously. The Department of Energy transferred the space battery program from Ohio to Argonne in 2002 because of security concerns.

The amount of radioactive plutonium in the RTG is about one-third the amount on board the Cassini–Huygens probe when it launched in 1997. That Cassini launch was protested by some. The United States Department of Energy estimated the chances of a New Horizons launch accident that would release radiation into the atmosphere at 1 in 350, and monitored the launch[53] as it always does when RTGs are involved. It was estimated that a worst-case scenario of total dispersal of on-board plutonium would spread the equivalent radiation of 80% the average annual dosage in North America from background radiation over an area with a radius of 105 km (65 mi).[54]

The spacecraft carries two computer systems: the Command and Data Handling system and the Guidance and Control processor. Each of the two systems is duplicated for redundancy, for a total of four computers. The processor used for its flight computers is the Mongoose-V, a 12 MHz radiation-hardened version of the MIPS R3000CPU. Multiple redundant clocks and timing routines are implemented in hardware and software to help prevent faults and downtime. To conserve heat and mass, spacecraft and instrument electronics are housed together in IEMs (integrated electronics modules). There are two redundant IEMs. Including other functions such as instrument and radio electronics, each IEM contains 9boards.[55] The software of the probe runs on Nucleus RTOS operating system.[56]

There have been two "safing" events, that sent the spacecraft into safe mode:

On March 19, 2007 the Command and Data Handling computer experienced an uncorrectable memory error and rebooted itself, causing the spacecraft to go into safe mode. The craft fully recovered within two days, with some data loss on Jupiter's magnetotail. No impact on the subsequent mission was expected.[57]

On July 4, 2015 there was a CPU safing event caused by over assignment of commanded science operations.[58][59]

Communication with the spacecraft is via X band. The craft had a communication rate of 7004380000000000000♠38 kbit/s at Jupiter; at Pluto's distance, a rate of approximately 7003100000000000000♠1 kbit/s per transmitter is expected. Besides the low data rate, Pluto's distance also causes a latency of about 4.5 hours (one-way). The 70 m (230 ft) NASA Deep Space Network (DSN) dishes are used to relay commands once it is beyond Jupiter. The spacecraft uses dual modular redundancy transmitters and receivers, and either right- or left-hand circular polarization. The downlink signal is amplified by dual redundant 12-watt traveling-wave tube amplifiers (TWTAs) mounted on the body under the dish. The receivers are new, low-power designs. The system can be controlled to power both TWTAs at the same time, and transmit a dual-polarized downlink signal to the DSN that nearly doubles the downlink rate. DSN tests early in the mission with this dual polarization combining technique were successful, and the capability is now considered operational (when the spacecraft power budget permits both TWTAs to be powered).

In addition to the high-gain antenna, there are two backup low-gain antennas and a medium-gain dish. The high-gain dish has a Cassegrain reflector layout, composite construction, and a 2.1-meter (7 ft) diameter providing over 7001420000000000000♠42 dBi of gain, has a half-power beam width of about a degree. The prime-focus, medium-gain antenna, with a 0.3-meter (1 ft) aperture and 10° half-power beam width, is mounted to the back of the high-gain antenna's secondary reflector. The forward low-gain antenna is stacked atop the feed of the medium-gain antenna. The aft low-gain antenna is mounted within the launch adapter at the rear of the spacecraft. This antenna was used only for early mission phases near Earth, just after launch and for emergencies if the spacecraft had lost attitude control.

New Horizons recorded scientific instrument data to its solid-state memory buffer at each encounter, then transmitted the data to Earth. Data storage is done on two low-power solid-state recorders (one primary, one backup) holding up to 7000800000000000000♠8 gigabytes each. Because of the extreme distance from Pluto and the Kuiper belt, only one buffer load at those encounters can be saved. This is because New Horizons would require approximately 16 months after leaving the vicinity of Pluto to transmit the buffer load back to Earth.[60] At Pluto's distance, radio signals from the space probe back to Earth took four hours and 25 minutes to traverse 4.7 billion km of space.[61]

Part of the reason for the delay between the gathering of and transmission of data is that all of the New Horizons instrumentation is body-mounted. In order for the cameras to record data, the entire probe must turn, and the one-degree-wide beam of the high-gain antenna was not pointing toward Earth. Previous spacecraft, such as the Voyager program probes, had a rotatable instrumentation platform (a "scan platform") that could take measurements from virtually any angle without losing radio contact with Earth. New Horizons was mechanically simplified to save weight, shorten the schedule, and improve reliability during its 15-year lifetime.

The Voyager 2 scan platform jammed at Saturn, and the demands of long time exposures at outer planets led to a change of plans such that the entire probe was rotated to make photos at Uranus and Neptune, similar to how New Horizons rotated.

New Horizons carries seven instruments: three optical instruments, two plasma instruments, a dust sensor and a radio science receiver/radiometer. The instruments are to be used to investigate the global geology, surface composition, surface temperature, atmospheric pressure, atmospheric temperature and escape rate of Pluto and its moons. The rated power is 7001210000000000000♠21 watts, though not all instruments operate simultaneously.[62] In addition, New Horizons has an Ultrastable Oscillator subsystem, which may be used to study and test the Pioneer anomaly towards the end of the spacecraft's life.[63]

The Long-Range Reconnaissance Imager (LORRI) is a long-focal-length imager designed for high resolution and responsivity at visible wavelengths. The instrument is equipped with a 1024×1024 pixel by 12-bits-per-pixel monochromatic CCD imager giving a resolution of 5μrad (~1arcsec).[64] The CCD is chilled far below freezing by a passive radiator on the antisolar face of the spacecraft. This temperature differential requires insulation, and isolation from the rest of the structure. The 208.3 mm (8.20 in) aperture Ritchey–Chretien mirrors and metering structure are made of silicon carbide, to boost stiffness, reduce weight, and prevent warping at low temperatures. The optical elements sit in a composite light shield, and mount with titanium and fiberglass for thermal isolation. Overall mass is 8.6 kg (19 lb), with the optical tube assembly (OTA) weighing about 5.6 kg (12 lb),[65] for one of the largest silicon-carbide telescopes flown at the time (now surpassed by Herschel). For viewing on public web sites the 12-bit per pixel LORRI images are converted to 8-bit per pixel JPEG images.[64] These public images do not contain the full dynamic range of brightness information available from the raw LORRI images files.[64]

Solar Wind Around Pluto (SWAP) is a toroidal electrostatic analyzer and retarding potential analyzer (RPA), that makes up one of the two instruments comprising New Horizons'Plasma and high-energy particle spectrometer suite (PAM), the other being PEPSSI. SWAP measures particles of up to 6.5keV and, because of the tenuous solar wind at Pluto's distance, the instrument is designed with the largest aperture of any such instrument ever flown.[67]

Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) is a time of flightion and electron sensor that makes up one of the two instruments comprising New Horizons' plasma and high-energy particle spectrometer suite (PAM), the other being SWAP. Unlike SWAP, which measures particles of up to 6.5keV, PEPSSI goes up to 1MeV.[67]

Alice is an ultraviolet imaging spectrometer that is one of two photographic instruments comprising New Horizons' Pluto Exploration Remote Sensing Investigation (PERSI); the other being the Ralph telescope. It resolves 1,024wavelength bands in the far and extreme ultraviolet (from 50–6993180000000000000♠180 nm), over 32view fields. Its goal is to determine the composition of Pluto's atmosphere. This Alice instrument is derived from another Alice aboard ESA's Rosetta spacecraft.[67]

The Ralph telescope, 75 mm[68] in aperture, is one of two photographic instruments that make up New Horizons' Pluto Exploration Remote Sensing Investigation (PERSI), with the other being the Alice instrument. Ralph has two separate channels: MVIC (Multispectral Visible Imaging Camera), a visible-light CCD imager with broadband and color channels; and LEISA (Linear Etalon Imaging Spectral Array), a near-infrared imaging spectrometer. LEISA is derived from a similar instrument on the Earth Observing-1 spacecraft. Ralph was named after Alice's husband on The Honeymooners, and was designed after Alice.[69]

On June 23, 2017, NASA announced that it has renamed the LEISA instrument to the "Lisa Hardaway Infrared Mapping Spectrometer" in honor of Lisa Hardaway, the Ralph program manager at Ball Aerospace, who died in January 2017 at age 50.[70]

The Venetia Burney Student Dust Counter (VBSDC), built by students at the University of Colorado Boulder, is operating periodically to make dust measurements.[71][72] It consists of a detector panel, about 460 mm × 300 mm (18 in × 12 in), mounted on the anti-solar face of the spacecraft (the ram direction), and an electronics box within the spacecraft. The detector contains fourteen polyvinylidene difluoride (PVDF) panels, twelve science and two reference, which generate voltage when impacted. Effective collecting area is 0.125 m2 (1.35 sq ft). No dust counter has operated past the orbit of Uranus; models of dust in the outer Solar System, especially the Kuiper belt, are speculative. The VBSDC is always turned on measuring the masses of the interplanetary and interstellar dust particles (in the range of nano- and picograms) as they collide with the PVDF panels mounted on the New Horizons spacecraft. The measured data is expected to greatly contribute to the understanding of the dust spectra of the Solar System. The dust spectra can then be compared with those from observations of other stars, giving new clues as to where Earth-like planets can be found in the universe. The dust counter is named for Venetia Burney, who first suggested the name "Pluto" at the age of 11. A thirteen-minute short film about the VBSDC garnered an Emmy Award for student achievement in 2006.[73]

The Radio Science Experiment (REX) used an ultrastable crystal oscillator (essentially a calibrated crystal in a miniature oven) and some additional electronics to conduct radio science investigations using the communications channels. These are small enough to fit on a single card. Because there are two redundant communications subsystems, there are two, identical REX circuit boards.

Launch of New Horizons. The Atlas V rocket on the launchpad (left) and lift off from Cape Canaveral.

On September 24, 2005, the spacecraft arrived at the Kennedy Space Center on board a C-17 Globemaster III for launch preparations.[74] The launch of New Horizons was originally scheduled for January 11, 2006, but was initially delayed until January 17, 2006, to allow for borescope inspections of the Atlas V's kerosene tank. Further delays related to low cloud ceiling conditions downrange, and high winds and technical difficulties—unrelated to the rocket itself—prevented launch for a further two days.[75][76]

The probe finally lifted off from Pad 41 at Cape Canaveral Air Force Station, Florida, directly south of Space ShuttleLaunch Complex 39, at 19:00 UTC on January 19, 2006.[77][78] The Centaur second stage ignited at 19:04:43 UTC and burned for 5 minutes 25 seconds. It reignited at 19:32 UTC and burned for 9 minutes 47 seconds. The ATKStar 48B third stage ignited at 19:42:37 UTC and burned for 1 minute 28 seconds.[79] Combined, these burns successfully sent the probe on a solar-escape trajectory at 16.26 kilometers per second (58,536 km/h; 36,373 mph).[80]New Horizons took only nine hours to pass the Moon's orbit.[81] Although there were backup launch opportunities in February 2006 and February 2007, only the first twenty-three days of the 2006 window permitted the Jupiter flyby. Any launch outside that period would have forced the spacecraft to fly a slower trajectory directly to Pluto, delaying its encounter by five to six years.[82]

The probe was launched by a Lockheed Martin Atlas V 551 rocket, with a third stage added to increase the heliocentric (escape) speed. This was the first launch of the Atlas V 551 configuration, which uses five solid rocket boosters, and the first Atlas V with a third stage. Previous flights had used zero, two, or three solid boosters, but never five. The vehicle, AV-010, weighed 573,160 kilograms (1,263,600 lb) at lift-off,[79] and had earlier been slightly damaged when Hurricane Wilma swept across Florida on October 24, 2005. One of the solid rocket boosters was hit by a door. The booster was replaced with an identical unit, rather than inspecting and requalifying the original.[83]

The launch was dedicated to the memory of launch conductor Daniel Sarokon, who was described by space program officials as one of the most influential people in the history of space travel.[84]

On January 28 and 30, 2006, mission controllers guided the probe through its first trajectory-correction maneuver (TCM), which was divided into two parts (TCM-1A and TCM-1B). The total velocity change of these two corrections was about 18 meters per second (65 km/h; 40 mph). TCM-1 was accurate enough to permit the cancellation of TCM-2, the second of three originally scheduled corrections.[85] On March 9, 2006, controllers performed TCM-3, the last of three scheduled course corrections. The engines burned for 76 seconds, adjusting the spacecraft's velocity by about 1.16 m/s (4.2 km/h; 2.6 mph).[86] Further trajectory maneuvers were not needed until September 25, 2007 (seven months after the Jupiter flyby), when the engines were fired for 15 minutes and 37 seconds, changing the spacecraft's velocity by 2.37 m/s (8.5 km/h; 5.3 mph),[87] followed by another TCM, almost three years later on June 30, 2010, that lasted 35.6 seconds, when New Horizons had already reached the halfway point (in time traveled) to Pluto.[88]

During the week of February 20, 2006, controllers conducted initial in-flight tests of three onboard science instruments, the Alice ultraviolet imaging spectrometer, the PEPSSI plasma-sensor, and the LORRI long-range visible-spectrum camera. No scientific measurements or images were taken, but instrument electronics, and in the case of Alice, some electromechanical systems were shown to be functioning correctly.[89]

On April 7, 2006, the spacecraft passed the orbit of Mars, moving at roughly 21 km/s (76,000 km/h; 47,000 mph) away from the Sun at a solar distance of 243 million kilometers.[90][91][92]

Because of the need to conserve fuel for possible encounters with Kuiper belt objects subsequent to the Pluto flyby, intentional encounters with objects in the asteroid belt were not planned. After launch, the New Horizons team scanned the spacecraft's trajectory to determine if any asteroids would, by chance, be close enough for observation. In May 2006 it was discovered that New Horizons would pass close to the tiny asteroid 132524 APL on June 13, 2006. Closest approach occurred at 4:05 UTC at a distance of 101,867 km (63,297 mi). The asteroid was imaged by Ralph (use of LORRI was not possible because of proximity to the Sun), which gave the team a chance to test Ralph's capabilities, and make observations of the asteroid's composition as well as light and phase curves. The asteroid was estimated to be 2.5 km (1.6 mi) in diameter.[93][94][95] The spacecraft successfully tracked the rapidly moving asteroid over June 10–12, 2006.

The first images of Pluto from New Horizons were acquired September 21–24, 2006, during a test of LORRI. They were released on November 28, 2006.[96] The images, taken from a distance of approximately 4.2 billion km (2.6 billion mi; 28 AU), confirmed the spacecraft's ability to track distant targets, critical for maneuvering toward Pluto and other Kuiper belt objects.

New Horizons used LORRI to take its first photographs of Jupiter on September 4, 2006, from a distance of 291 million kilometers (181 million miles).[97] More detailed exploration of the system began in January 2007 with an infrared image of the moon Callisto, as well as several black-and-white images of Jupiter itself.[98]New Horizons received a gravity assist from Jupiter, with its closest approach at 05:43:40 UTC on February 28, 2007, when it was 2.3 million kilometers (1.4 million miles) from Jupiter. The flyby increased New Horizons' speed by 4 km/s (14,000 km/h; 9,000 mph), accelerating the probe to a velocity of 23 km/s (83,000 km/h; 51,000 mph) relative to the Sun and shortening its voyage to Pluto by three years.[99]

The flyby was the center of a four-month intensive observation campaign lasting from January to June. Being an ever-changing scientific target, Jupiter has been observed intermittently since the end of the Galileo mission in September 2003. Knowledge about Jupiter benefited from the fact that New Horizons' instruments were built using the latest technology, especially in the area of cameras, representing a significant improvement over Galileo's cameras, which were modified versions of Voyager cameras, which, in turn, were modified Mariner cameras. The Jupiter encounter also served as a shakedown and dress rehearsal for the Pluto encounter. Because Jupiter is much closer to Earth than Pluto, the communications link can transmit multiple loadings of the memory buffer; thus the mission returned more data from the Jovian system than it was expected to transmit from Pluto.[100]

One of the main goals during the Jupiter encounter was observing its atmospheric conditions and analyzing the structure and composition of its clouds. Heat-induced lightning strikes in the polar regions and "waves" that indicate violent storm activity were observed and measured. The Little Red Spot, spanning up to 70% of Earth's diameter, was imaged from up close for the first time.[99] Recording from different angles and illumination conditions, New Horizons took detailed images of Jupiter's faint ring system, discovering debris left over from recent collisions within the rings or from other unexplained phenomena. The search for undiscovered moons within the rings showed no results. Travelling through Jupiter's magnetosphere, New Horizons collected valuable particle readings.[99] "Bubbles" of plasma that are thought to be formed from material ejected by the moon Io, were noticed in the magnetotail.[101]

The four largest moons of Jupiter were in poor positions for observation; the necessary path of the gravity-assist maneuver meant that New Horizons passed millions of kilometers from any of the Galilean moons. Still, its instruments were intended for small, dim targets, so they were scientifically useful on large, distant moons. Emphasis was put on Jupiter's innermost Galilean moon, Io, whose active volcanoes shoot out tons of material into Jupiter's magnetosphere, and further. Out of eleven observed eruptions, three were seen for the first time. That of Tvashtar reached an altitude of up to 330 km (210 mi). The event gave scientists an unprecedented look into the structure and motion of the rising plume and its subsequent fall back to the surface. Infrared signatures of a further 36 volcanoes were noticed.[99] Callisto's surface was analyzed with LEISA, revealing how lighting and viewing conditions affect infrared spectrum readings of its surface water ice.[102] Minor moons such as Amalthea had their orbit solutions refined. The cameras determined their positions, acting as "reverse optical navigation".

Jovian moons imaged by New Horizons

Io imaged on February 28. The feature near the north pole of the moon is a 290 km (180 mi) high plume from the volcano Tvashtar.

Europa imaged on February 27 from a distance of 3.1 million km (1.9 million mi). Image scale is 15 km per pixel (9.3 mi/px).

Ganymede imaged on February 27, 2007, from a distance of 3.5 million km (2.2 million mi). Image scale is 17 km per pixel (11 mi/px).

Callisto imaged on February 27 from a distance of 4.7 million km (2.9 million mi).

After passing Jupiter, New Horizons spent most of its journey towards Pluto in hibernation mode: redundant components as well as guidance and control systems were shut down to extend their life cycle, decrease operation costs and free the Deep Space Network for other missions.[103] During hibernation mode, the onboard computer monitored the probe's systems and transmitted a signal back to Earth: a "green" code if everything was functioning as expected or a "red" code if mission control's assistance was needed.[103] The probe was activated for about two months a year so that the instruments could be calibrated and the systems checked. The first hibernation mode cycle started on June 28, 2007,[103] the second cycle began on December 16, 2008,[104] the third cycle on August 27, 2009,[105] and the fourth cycle on August 29, 2014 after a 10-week test.[106]

New Horizons crossed the orbit of Saturn on June 8, 2008,[107] and Uranus on March 18, 2011.[108] After astronomers announced the discovery of two new moons in the Pluto system, Kerberos and Styx, mission planners started contemplating the possibility of the probe running into unseen debris and dust left over from ancient collisions between the moons. A study based on 18 months of computer simulations, Earth-based telescope observations and occultations of the Pluto system revealed that the possibility of a catastrophic collision with debris or dust was less than 0.3% on the probe's scheduled course.[109][110] If the hazard increased, New Horizons could have used one of two possible contingency plans, the so-called SHBOTs (Safe Haven by Other Trajectories): the probe could have continued on its present trajectory with the antenna facing the incoming particles so the more vital systems would be protected, or, it could have positioned its antenna to make a course correction that would take it just 3000 km from the surface of Pluto where it was expected that the atmospheric drag would clean the surrounding space of possible debris.[110]

While in hibernation mode in July 2012, New Horizons started gathering scientific data with SWAP, PEPSSI and VBSDC. Although it was originally planned to activate just the VBSDC, other instruments were powered on the initiative of principal investigator Alan Stern who decided they could use the opportunity to collect valuable heliospheric data. Before activating the other two instruments, ground tests were conducted to make sure that the expanded data gathering in this phase of the mission would not limit available energy, memory and fuel in the future and that all systems are functioning during the flyby.[111] The first set of data was transmitted in January 2013 during a three-week activation from hibernation. The command and data handling software was updated to address the problem of computer resets.[112]

Other possible targets were Neptune trojans. The probe's trajectory to Pluto passed near Neptune's trailing Lagrange point ("L5"), which may host hundreds of bodies in 1:1 resonance. In late 2013, New Horizons passed within 1.2 AU (180,000,000 km; 110,000,000 mi) of the high-inclination L5 Neptune trojan 2011 HM102,[113] which was identified shortly before by the New Horizons KBO Search survey team while searching for more distant objects for New Horizons to fly by after its 2015 Pluto encounter. At that range, 2011 HM102 would have been bright enough to be detectable by New Horizons' LORRI instrument; however, the New Horizons team eventually decided that they would not target 2011 HM102 for observations because the preparations for the Pluto approach took precedence.[114]

Images from July 1 to 3, 2013 by LORRI were the first by the probe to resolve Pluto and Charon as separate objects.[115] On July 14, 2014, mission controllers performed a sixth trajectory-correction maneuver (TCM) since its launch to enable the craft to reach Pluto.[116] Between July 19–24, 2014, New Horizons' LORRI snapped 12 images of Charon revolving around Pluto, covering almost one full rotation at distances ranging from about 429 to 422 million kilometers (267,000,000 to 262,000,000 mi).[117] In August 2014, astronomers made high-precision measurements of Pluto's location and orbit around the Sun using the Atacama Large Millimeter/submillimeter Array (ALMA) to help NASA's New Horizons spacecraft accurately home in on Pluto.[118] On December 6, 2014, mission controllers sent a signal for the craft to "wake up" from its final Pluto-approach hibernation and begin regular operations. The craft's response that it was "awake" arrived to Earth on December 7, 2014, at 02:30 UTC.[119][120][121]

Pluto and Charon photographed on April 9 (left) by Ralph and on June 29 (right) by LORRI

Distant-encounter operations at Pluto began on January 4, 2015.[122] At this date images of the targets with the onboard LORRI imager plus Ralph telescope would only be a few pixels in width. Investigators began taking Pluto and background starfield images to assist mission navigators in the design of course-correcting engine maneuvers that would precisely modify the trajectory of New Horizons to aim the approach. On January 15, 2015, NASA gave a brief update of the timeline of the approach and departure phases.[123]

On February 12, 2015, NASA released new images of Pluto (taken from January 25 to 31) from the approaching probe.[124][125]New Horizons was more than 203 million kilometers (126,000,000 mi) away from Pluto when it began taking the photos, which showed Pluto and its largest moon, Charon. The exposure time was too short to see Pluto's smaller, much fainter, moons.

Investigators compiled a series of images of the moons Nix and Hydra taken from January 27 through February 8, 2015, beginning at a range of 201 million kilometers (125,000,000 mi).[126] Pluto and Charon appear as a single overexposed object at the center. The right side image has been processed to remove the background starfield. The yet smaller two moons, Kerberos and Styx were seen on photos taken on April 25.[127] Starting May 11 a hazard search was performed, by looking for unknown objects that could be a danger to the spacecraft, such as rings or more moons, which were possible to avoid by a course change.[128]

Also in regards to the approach phase during January 2015, on August 21, 2012, the team announced that they would spend mission time attempting long-range observations of the Kuiper belt object temporarily designated VNH0004 (now designated 2011 KW48), when the object was at a distance from New Horizons of 75 gigameters (0.50 AU).[129] The object would be too distant to resolve surface features or take spectroscopy, but it would be able to make observations that cannot be made from Earth, namely a phase curve and a search for small moons. A second object was planned to be observed in June 2015, and a third in September after the flyby; the team hoped to observe a dozen such objects through 2018.[129] On April 15, 2015, Pluto was imaged showing a possible polar cap.[130]

On July 4, 2015, New Horizons experienced a software anomaly and went into safe mode, preventing the spacecraft from performing scientific observations until engineers could resolve the problem.[131][132] On July 5, NASA announced that the problem was determined to be a timing flaw in a command sequence used to prepare the spacecraft for its flyby, and the spacecraft would resume scheduled science operations on July 7. The science observations lost because of the anomaly were judged to have no impact on the mission's main objectives and minimal impact on other objectives.[133]

The timing flaw consisted of performing two tasks simultaneously—compressing previously acquired data to release space for more data, and making a second copy of the approach command sequence—that together overloaded the spacecraft's primary computer. After the overload was detected, the spacecraft performed as designed: it switched from the primary computer to the backup computer, entered safe mode, and sent a distress call back to Earth. The distress call was received the afternoon of July 4, which alerted engineers that they needed to contact the spacecraft to get more information and resolve the issue. The resolution was that the problem happened as part of preparations for the approach, and was not expected to happen again because no similar tasks were planned for the remainder of the encounter.[133][134]

Alan Stern and the New Horizons team celebrate after the spacecraft successfully completed its flyby of Pluto.

The closest approach of the New Horizons spacecraft to Pluto occurred at 11:49 UTC on July 14, 2015 at a range of 12,472 km (7,750 mi) from the surface[135] and 13,658 km (8,487 mi) from the center of Pluto. Telemetry data confirming a successful flyby and a healthy spacecraft were received on Earth from the vicinity of the Pluto system on July 15, 2015, 00:52:37 UTC,[136] after 22 hours of planned radio silence due to the spacecraft being pointed toward the Pluto system. Mission managers estimated a one in 10,000 chance that debris could have destroyed it during the flyby, preventing it from sending data to Earth.[137] The first details of the encounter were received the next day, but the download of the complete data set took just over 15 months,[18] and analysis of the data will take longer.

The mission's science objectives are grouped in three distinct priorities. The "primary objectives" are required; the "secondary objectives" are expected to be met but are not demanded. The "tertiary objectives" are desired. These objectives may be attempted, though they may be skipped in favor of the above objectives. An objective to measure any magnetic field of Pluto was dropped. A magnetometer instrument could not be implemented within a reasonable mass budget and schedule, and SWAP and PEPSSI could do an indirect job detecting some magnetic field around Pluto.[138]

Pluto's "encounter hemisphere" viewed by New Horizons on July 13, 2015

Pluto's Charon-facing opposing hemisphere viewed on July 11, 2015

New Horizons passed within 12,500 km (7,800 mi) of Pluto, with this closest approach on July 14, 2015 at 11:50 UTC. New Horizons had a relative velocity of 13.78 km/s (49,600 km/h; 30,800 mph) at its closest approach, and came as close as 28,800 km (17,900 mi) to Charon. Starting 3.2 days before the closest approach, long-range imaging included the mapping of Pluto and Charon to 40 km (25 mi) resolution. This is half the rotation period of the Pluto–Charon system and allowed imaging of all sides of both bodies. Close range imaging was repeated twice per day in order to search for surface changes caused by localized snow fall or surface cryovolcanism. Because of Pluto's tilt, a portion of the northern hemisphere would be in shadow at all times. During the flyby, engineers expected LORRI to be able to obtain select images with resolution as high as 50 m per pixel (160 ft/px) if closest distance were around 12,500 km, and MVIC was expected to obtain four-color global dayside maps at 1.6 km (1 mi) resolution. LORRI and MVIC attempted to overlap their respective coverage areas to form stereo pairs. LEISA obtained hyperspectral near-infrared maps at 7 km/px (4.3 mi/px) globally and 0.6 km/px (0.37 mi/px) for selected areas.

Patterns of blue-gray ridges and reddish material observed in the Tartarus Dorsa region on July 14

Meanwhile, Alice characterized the atmosphere, both by emissions of atmospheric molecules (airglow), and by dimming of background stars as they pass behind Pluto (occultation). During and after closest approach, SWAP and PEPSSI sampled the high atmosphere and its effects on the solar wind. VBSDC searched for dust, inferring meteoroid collision rates and any invisible rings. REX performed active and passive radio science. The communications dish on Earth measured the disappearance and reappearance of the radio occultation signal as the probe flew by behind Pluto. The results resolved Pluto's diameter (by their timing) and atmospheric density and composition (by their weakening and strengthening pattern). (Alice can perform similar occultations, using sunlight instead of radio beacons.) Previous missions had the spacecraft transmit through the atmosphere, to Earth ("downlink"). Pluto's mass and mass distribution were evaluated by the gravitational tug on the spacecraft. As the spacecraft speeds up and slows down, the radio signal exhibited a Doppler shift. The Doppler shift was measured by comparison with the ultrastable oscillator in the communications electronics.

Reflected sunlight from Charon allowed some imaging observations of the nightside. Backlighting by the Sun gave an opportunity to highlight any rings or atmospheric hazes. REX performed radiometry of the nightside.

Initial predictions envisioned Kerberos as a relatively large and massive object whose dark surface led to it having a faint reflection. This proved to be wrong as images obtained by New Horizons on July 14 and sent back to Earth in October 2015 revealed an object just 8 km (5.0 mi) across with a highly reflective surface suggesting the presence of relatively clean water ice.[139]

View of Pluto as New Horizons left the system, catching the Sun's rays passing through Pluto's atmosphere, forming a ring

Soon after the Pluto flyby, in July 2015, New Horizons reported that the spacecraft was healthy, its flight path was within the margins, and science data of the Pluto–Charon system had been recorded.[140][141] The spacecraft's immediate task was to begin returning the 6.25 gigabytes of information collected.[18] The free-space path loss at its distance of 4.5 light-hours (3,017,768,400 km) is approximately 303 dB at 7 GHz. Using the high gain antenna and transmitting at full power, New Horizons' EIRP is +83 dBm, and at this distance the signal reaching Earth is −220 dBm. The received signal level (RSL) using one, un-arrayed Deep Space Network antenna with 72 dBi of forward gain equals −148 dBm.[142] Because of the extremely low RSL, it could only transmit data at 1 to 2 kilobits per second.[143]

By March 30, 2016, New Horizons had reached the halfway point of transmitting this data.[144] The transfer was completed on October 25, 2016 at 21:48 UTC, when the last piece of data—part of a Pluto–Charon observation sequence by the Ralph/LEISA imager—was received by the Johns Hopkins University Applied Physics Laboratory.[18][145]

The New Horizons team requested, and received, a mission extension through 2021 to explore additional Kuiper belt objects (KBOs). During this Kuiper Belt Extended Mission (KEM), the spacecraft will perform a close fly-by of (486958) 2014 MU69 and conduct more distant observations on an additional two dozen objects.[148][149][150]

Mission planners searched for one or more additional Kuiper belt objects (KBOs) of the order of 50–100 km (31–62 mi) in diameter as targets for flybys similar to the spacecraft's Plutonian encounter, but, despite the large population of KBOs, many factors limit the number of possible targets. Because the flight path is determined by the Pluto flyby, and the probe only has 33 kilograms of hydrazine remaining, the object to be visited needs to be within a cone, extending from Pluto, of less than a degree's width. This ruled out any possibility for a flyby of Eris, a trans-Neptunian object comparable in size to Pluto.[151] It will also need to be within 55AU, because beyond 55AU, the communications link will become too weak, and the RTG power output will have decayed significantly enough to hinder observations. Desirable KBOs would be well over 50 km (30 mi) in diameter, neutral in color (to compare with the reddish Pluto), and, if possible, have a moon that imparts a wobble. After a search along New Horizon's flight path using the Hubble Space Telescope, only three KBOs were found in range, and one of those objects was later dropped from consideration.[152]

In 2011 a dedicated search for suitable KBOs using ground telescopes was started by mission scientists. Large ground telescopes with wide-field cameras, notably the twin 6.5-meter Magellan Telescopes in Chile, the 8.2-meter Subaru Observatory in Hawaii, and the Canada–France–Hawaii Telescope[113][153] were used to search for potential targets. Through the citizen-science project, the public helped to scan telescopic images for possible suitable mission candidates by participating in the Ice Hunters project.[154][155][156][157][158] The ground-based search resulted in the discovery of about 143 KBOs of potential interest,[159] but none of these were close enough to the flight path of New Horizons.[153] Only the Hubble Space Telescope was deemed likely to find a suitable target in time for a successful KBO mission.[160] On June 16, 2014, time on Hubble was granted.[161] Hubble has a much greater ability to find suitable KBOs than ground telescopes. The probability that a target for New Horizons would be found was estimated beforehand at about 95%.[162]

On October 15, 2014, it was revealed that Hubble's search had uncovered three potential targets,[163][164][165][166][167] temporarily designated PT1 ("potential target 1"), PT2 and PT3 by the New Horizons team. All are objects with estimated diameters in the 30–55 km (19–34 mi) range, too small to be seen by ground telescopes, at distances from the Sun of 43–44 AU, which would put the encounters in the 2018–2019 period.[164] The initial estimated probabilities that these objects are reachable within New Horizons' fuel budget are 100%, 7%, and 97%, respectively.[164] All are members of the "cold" (low-inclination, low-eccentricity) classical Kuiper belt, and thus very different from Pluto. PT1 (given the temporary designation "1110113Y" on the HST web site[168]), the most favorably situated object, is magnitude 26.8, 30–45 km (19–28 mi) in diameter, and will be encountered around January 2019.[169] A course change to reach it required about 35% of New Horizons' available trajectory-adjustment fuel supply. A mission to PT3 was in some ways preferable, in that it is brighter and therefore probably larger than PT1, but the greater fuel requirements to reach it would have left less for maneuvering and unforeseen events.[164] Once sufficient orbital information was provided, the Minor Planet Center gave provisional designations to the three target KBOs: 2014 MU69 (PT1), 2014 OS393 (PT2), and 2014 PN70 (PT3). By the fall of 2014, a possible fourth target, 2014 MT69, had been eliminated by follow-up observations. PT2 was out of the running before the Pluto flyby.[170][171] The spacecraft will also study almost 20 KBOs from afar.[172]

On August 28, 2015, (486958) 2014 MU69 (PT1) was chosen as the flyby target. The necessary course adjustment was performed with four engine firings between October 22 and November 4, 2015.[173][174] The flyby is scheduled for January 1, 2019.[175][176] Funding was secured on July 1, 2016.[149]

Aside from its flyby of (486958) 2014 MU69, the extended mission for New Horizons calls for the spacecraft to conduct observations of, and look for ring systems around, between 25 and 35 different KBOs.[177] In addition, it will continue to study the gas, dust and plasma composition of the Kuiper belt before the mission extension ends in 2021.[148][150]

On November 2, 2015, New Horizons imaged KBO 15810 Arawn with the LORRI instrument from 280 million km away (170 million mi; 1.9 AU), showing the shape of the object and one or two details.[178] This KBO was again imaged by the LORRI instrument on April 7–8, 2016, from a distance of 111 million km (69 million mi; 0.74 AU). The new images allowed the science team to further refine the location of 15810 Arawn to within 1,000 km (620 mi) and to determine its rotational period of 5.47 hours.[179][180]

On December 5, 2017, when New Horizons was 40.9 AU from Earth, a calibration image of the Wishing Well cluster marked the most distant image from Earth ever taken by a spacecraft (breaking the 27-year record set by Voyager 1's famous Pale Blue Dot). Two hours later, New Horizons surpassed its own record, imaging the Kuiper belt objects 2012 HZ84 and 2012 HE85 from a distance of 0.50 and 0.34 AU, respectively. These are the closest images of a Kuiper belt object besides Pluto as of February 2018[update].[182][183]

Science objectives of the 2018-2019 flyby include characterizing the geology and morphology of 2014 MU69 (nicknamed Ultima Thule), mapping the surface composition (searching for ammonia, carbon monoxide, methane, and water ice). Searches will be conducted for orbiting moonlets, a coma, rings, and the surrounding environment.[184] Additional objectives include:[185]

Mapping the surface geology to learn how it formed and has evolved

Measuring the surface temperature

Mapping the 3D surface topography and surface composition to learn how it is similar to and different from comets like 67P and dwarf planets such as Pluto

2014 MU69 is the first object to be targeted for a flyby that was discovered after the spacecraft was launched.[186]New Horizons is planned to come within 3,500 km (2,200 mi) of 2014 MU69, three times closer than the spacecraft's earlier encounter with Pluto. Images with a resolution of up to 30 m (98 ft) are expected.[187]

The new mission began on October 22, 2015, when New Horizons carried out the first in a series of four initial targeting maneuvers designed to send it toward 2014 MU69. The maneuver, which started at approximately 19:50 UTC and used two of the spacecraft's small hydrazine-fueled thrusters, lasted approximately 16 minutes and changed the spacecraft's trajectory by about 10 meters per second (33 ft/s). The remaining three targeting maneuvers took place on October 25, October 28, and November 4, 2015.[188][189]

The craft was brought out of its hibernation at approximately 00:33 UTCSCET on June 5, 2018 (06:12 UTC ERT),[a] in order to prepare for the approach phase.[191][192] After verifying its health status, the spacecraft transitioned from a spin-stabilized mode to a 3-axis-stabilized mode on August 13, 2018. The official approach phase began on August 16, 2018, and continues through December 24, 2018.[193] The first images from New Horizons were scheduled to be taken in early September 2018. If obstacles are detected, mission planners may opt to divert the spacecraft's trajectory as late as mid-December 2018.[184]

New Horizons made its first detection of 2014 MU69 on August 16, 2018, from a distance of 107 million mi (172 million km). At that time, 2014 MU69 was visible at magnitude 20, against a crowded stellar background in the direction of the constellation Sagittarius.[194][195]

The Core phase begins a week before the encounter, and continues for two days after the encounter. The majority of the science data will be collected within 48 hours of the closest approach in a phase called the Inner Core.[193] Closest approach will occur January 1, 2019, at 05:33 UTC,[196] at which point it will be 7012649254758838000♠43.4 AU from the Sun.[197] At this distance, the one-way transit time for radio signals between Earth and New Horizons will be 6 hours.[184]

After the encounter, preliminary data will be sent to Earth on January 1 and 2, 2019, to transmit high priority data. On January 9, New Horizons will return to a spin-stabilized mode, to prepare to send the remainder of its data back to Earth. This downlink is expected to continue through most of 2019.[193]

New Horizons has been called "the fastest spacecraft ever launched"[198] because it left Earth at 16.26 kilometers per second (58,536 km/h; 36,373 mph), faster than any other spacecraft to date.[80][199] It is also the first spacecraft launched directly into a solar escape trajectory, which requires an approximate speed while near Earth of 16.5 km/s (59,000 km/h; 37,000 mph),[b] plus additional delta-v to cover air and gravity drag, all to be provided by the launch vehicle.

However, it is not the fastest spacecraft to leave the Solar System. As of January 2018[update], this record is held by Voyager 1, traveling at 16.985 km/s (61,146 km/h; 37,994 mph) relative to the Sun.[147]Voyager 1 attained greater hyperbolic excess velocity than New Horizons thanks to gravity assists by Jupiter and Saturn. When New Horizons reaches the distance of 7013149597870700000♠100 AU, it will be travelling at about 13 km/s (47,000 km/h; 29,000 mph), around 4 km/s (14,000 km/h; 8,900 mph) slower than Voyager 1 at that distance.[200] Other spacecraft, such as the Helios probes, can also be measured as the fastest objects, because of their orbital speed relative to the Sun at perihelion: 68.7 km/s (247,000 km/h; 154,000 mph) for Helios-B. Because they remain in solar orbit, their specific orbital energy relative to the Sun is lower than New Horizons and other artificial objects escaping the Solar System.

New Horizons'Star 48B third stage is also on a hyperbolic escape trajectory from the Solar System, and reached Jupiter before the New Horizons spacecraft. The Star 48B was expected to cross Pluto's orbit on October 15, 2015.[201] Because it is not in controlled flight, it did not receive the correct gravity assist, and passed within 200 million km (120 million mi) of Pluto.[201] The Centaur second stage did not achieve solar escape velocity, and remains in a heliocentric orbit.[202]

April 6, 2001: New Horizons proposal submitted to NASA. It was one of five proposals submitted, which were later narrowed to two for Phase A study: POSSE (Pluto and Outer Solar System Explorer) and New Horizons. [203]

July 2015 to October 2016: Transmission of collected data back to Earth, and ongoing science discovery based on the observations. The bit rate of the downlink is limited to 1–2 kb/s,[143] so it took until October 25, 2016, to transmit all of the data.[18][238][239][240]

October 22 – November 4, 2015: Trajectory correction maneuver. Course adjustment towards the January 2019 flyby of 2014 MU69 was performed in a series of four thruster firings of 22 minutes each.[173][241]

November 2, 2015: Observation of KBO 15810 Arawn. Long-range observations from a distance of 170 million miles (1.8 AU), the closest ever for any Trans-Neptunian Object other than Pluto. More images were taken on April 7–8, 2016, at a range of 111 million miles (1.19 AU) as well.[242]

July 13–14, 2016: Observation of KBO 50000 Quaoar. Long-range observations from a distance of 1.3 billion miles (14 AU) gives mission scientists a different perspective in order to study the light-scattering properties of Quaoar's surface.[243]

February 1, 2017: Trajectory correction maneuver. A small course adjustment towards the January 2019 flyby of 2014 MU69 was performed with a 44-second thruster firing.[244][173]

2017–2020: Observations of Kuiper belt objects (KBOs). The probe will have opportunities to perform observations of 10 to 20 KBOs visible from the spacecraft's trajectory after the Pluto system flyby. Heliosphere data collection is expected to begin.[186][245][246]

December 9, 2017: Trajectory correction maneuver. This delays the arrival at 2014 MU69 by a few hours, optimizing coverage by ground-based radio telescopes.[247][248]

December 23, 2017 – June 4, 2018: Final hibernation period before the (KBO) 2014 MU69 encounter.[249][247]

August 2018 – March 2019: Distant observations of at least a dozen distant KBOs. Recovered by Subaru Telescope in 2014–2017, enabling New Horizons observations[177]

January 1, 2019: Flyby of Kuiper belt object 2014 MU69. • Flyby to occur at 05:33 UTC • Expected to be the outermost close encounter of any Solar System object.[196]

January 9, 2019: Switch from 3-axis mode to spin mode. This ends the 2014 MU69 flyby, marking the beginning of the downlink phase.[247]

2019-2020: Downlink of data from 2014 MU69 flyby. Predicted to take approximately 18 months.[247]

April 30, 2021: End of extended mission. It is expected that the mission will be extended further if the spacecraft remains operational.[247]

2020s: The probe may be able to fly by a second KBO. The probe is approaching 2014 MU69 along its rotational axis, which simplifies trajectory correction maneuvers, saving fuel that can be used to target another KBO.[250]

No earlier than 2026: Expected end of the mission, based on RTG plutonium decay. Heliosphere data collection expected to be intermittent if instrument power sharing is required.[251]

^Confirmation that New Horizons exited hibernation was received by ground stations at 06:12 UTC. Spacecraft Event Time is calculated by subtracting the one-way light-travel time (5 hours, 38 minutes, 38 seconds) from Earth-received time.[190]

^To escape the Sun the spacecraft needs a speed relative to the Sun of the square root of 2 times the speed of the Earth (29.78 km/s), or 42.1 km/s. Relative to the Earth this is just 12.3 km/s. But the kinetic energy when near the surface of the Earth must include the energy to exit the gravity well of the Earth, which requires a speed of about 11 km/s. The total speed needed is the square root of the sum of the squares of these two speeds.[citation needed]